Probing changes of dust properties along a chain of solar-type prestellar and protostellar cores in Taurus with NIKA

Astronomy and Astrophysics - Tập 604 - Trang A52 - 2017
A. Bracco1, P. Palmeirim2,3, P. André1, R. Adam4,5, P. A. R. Ade6, A. Bacmann7, A. Beelen8, A. Benoı̂t9, A. Bideaud9, N. Billot10, O. Bourrion5, M. Calvo Gomez9, J.-F. Cardoso5, G. Coiffard11, L. P. L. Colombo5, A. D’Addabbo12,9, F.–X. Désert7, P. Didelon1, S. Doyle6, J. Goupy9, V. Könyves1, C. Kramer10, G. Lagache2, S. Leclercq11, B. Maffei5, A. Maury1, P. Mauskopf6,13, F. Mayet5, A. Moneti9, F. Motte7, F. Pajot8, E. Pascale6, N. Peretto6, L. Perotto5, G. Pisano6, N. Ponthieu7, V. Revéret1, A. J. Rigby6, A. Ritacco10,5, L. Rodriguez1, C. Romero11, A. Roy1, F. Ruppin5, K. Schuster11, A. Sievers10, S. Triqueneaux9, C. Tucker6, R. Zylka11
1Laboratoire AIM, CEA/IRFU, CNRS/INSU, Université Paris Diderot, CEA-Saclay, 91191Gif-Sur-Yvette, France
2Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
3Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762, Porto, Portugal
4Laboratoire Lagrange, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Bd de l'Observatoire, CS 34229, 06304 Nice Cedex 4, France
5Laboratoire de Physique Subatomique et de Cosmologie, Université Grenoble Alpes, CNRS/IN2P3, 53 avenue des Martyrs, 38026 Grenoble, France
6Astronomy Instrumentation Group, University of Cardiff, Cardiff CF10 3XQ, UK
7Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
8Institut d'Astrophysique Spatiale (IAS), CNRS and Université Paris Sud, 91405 Orsay, France
9Institut Néel, CNRS and Université Grenoble Alpes, 38042 Grenoble, France
10Institut de RadioAstronomie Millimétrique (IRAM), 18012 Granada, Spain
11Institut de RadioAstronomie Millimétrique (IRAM), 38406 Grenoble, France
12Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro 5, 00185 Roma, Italy
13School of Earth and Space Exploration and Department of Physics, Arizona State University, Tempe, AZ, 85287, USA

Tóm tắt

The characterization of dust properties in the interstellar medium is key for understanding the physics and chemistry of star formation. Mass estimates are crucial to determine gravitational collapse conditions for the birth of new stellar objects in molecular clouds. However, most of these estimates rely on dust models that need further observational constraints to capture the relevant parameter variations depending on the local environment: from clouds to prestellar and protostellar cores. We present results of a new study of dust emissivity changes based on millimeter continuum data obtained with the NIKA camera at the IRAM-30 m telescope. Observing dust emission at 1.15 mm and 2 mm allows us to constrain the dust emissivity index, β, in the Rayleigh-Jeans tail of the dust spectral energy distribution far from its peak emission, where the contribution of other parameters (i.e. dust temperature) is more important. Focusing on the Taurus molecular cloud, one of the most famous low-mass star-forming regions in the Gould Belt, we analyze the emission properties of several distinct objects in the B213 filament. This subparsec-sized region is of particular interest since it is characterized by a collection ofevolutionary stages of early star formation: three prestellar cores, two Class 0/I protostellar cores and one Class II object. We are therefore able to compare dust properties among a sequence of sources that likely derive from the same parent filament. By means of the ratio of the two NIKA channel maps, we show that in the Rayleigh-Jeans approximation, βRJ varies among the objects: it decreases from prestellar cores (βRJ ~ 2) to protostellar cores (βRJ ~ 1) and the Class II object (βRJ ~ 0). For one prestellar and two protostellar cores, we produce a robust study using available Herschel data to constrain the dust temperature of the sources. By using the Abel transform inversion technique we derive accurate radial temperature profiles that allow us to obtain radial β profiles. We find systematic spatial variations of β in the protostellar cores that are not observed in the prestellar core. While in the former case β decreases toward the center (with β varying between 1 and 2), in the latter it remains constant (β = 2.4 ± 0.3). Moreover, the dust emissivity index appears anticorrelated with the dust temperature. We discuss the implication of these results in terms of dust grain evolution between pre- and protostellar cores.

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Astronomy and Astrophysics

Tập 604

A52

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